APAKAH MAKSUD SEMIDETACHED BINARY dalam CORSICA?
Bintang binari
Bintang binari adalah sistem bintang yang terdiri daripada dua bintang yang mengorbit di sekitar pusat massa yang sama. Bintang yang lebih besar dipanggil utama dan yang lainnya adalah bintang pengiringnya, datang / koʊmiːz /, atau sekunder. Sistem dua, tiga, empat, atau lebih banyak bintang dipanggil berbilang sistem bintang. Sistem ini, terutamanya apabila lebih jauh, sering muncul pada mata tanpa mata sebagai satu titik cahaya, dan kemudian dinyatakan sebagai dua kali ganda dengan cara lain. Penyelidikan sejak dua abad yang lalu menunjukkan bahawa separuh atau lebih bintang yang kelihatan adalah sebahagian daripada sistem bintang berbilang. Istilah bintang double sering digunakan secara sinonim dengan bintang binari; Walau bagaimanapun, bintang double juga boleh bermaksud bintang double optik. Beregu optik dipanggil kerana kedua-dua bintang kelihatan rapat di langit seperti yang dilihat dari Bumi; mereka hampir pada garis penglihatan yang sama. Walau bagaimanapun, "kedalaman" mereka hanya bergantung kepada kesan optik ini; bintang-bintang itu sendiri jauh dari satu sama lain dan tidak berkongsi sambungan fizikal. Bintang ganda boleh didedahkan sebagai optik dengan perbezaan dalam pengukuran paralaks mereka, gerakan yang betul, atau halaju radial.
Definisi semidetached binary dalam kamus Corsica
Takrif binari semidetached dalam kamus adalah sepasang bintang yang begitu rapat bersama sehingga perpindahan massa berlaku dari satu ke yang lain.
CORSICA BUKU YANG BERKAIT DENGAN «SEMIDETACHED BINARY»
Ketahui penggunaan
semidetached binary dalam pilihan bibliografi berikut. Buku yang berkait dengan
semidetached binary dan ekstrak ringkas dari yang sama untuk menyediakan konteks penggunaannya dalam kesusasteraan Corsica.
1
The Physical Universe: An Introduction to Astronomy
BOX 10.3 Semidetached Binaries The appearance of a semidetached binary in
which mass is transferred from a normal lobe-filling star to its companion
depends largely on the physical nature of the detached companion. (1) If the
detached ...
2
An Introduction to Close
Binary Stars
The mass ratio (secondary/primary) is q = 0.85. Orbit sizes for detached binaries
range from about 1 Ro up to those of resolved binaries (astronomical units, AUs).
Fig. 1.4. A semidetached binary system, with a mass ratio. 7.5 Types of binaries: ...
3
Zdenek Kopal's
Binary Star Legacy
For these three systems we obtained near-contact configurations, but it is also
possible that BL And might be a semidetached binary. Configuration ofCNAnd is
most probably either detached or semidetached, but our solutions are not
finished ...
Horst Drechsel, Miloslav Zejda,
2005
(b) A semidetached binary occurs when one member star swells up to fill or
overflow its Roche lobe. Gas can then escape from its distorted surface and flow
over to its neighbor, (c) A contact binary consists of two stars, both of which have
filled ...
5
100 Billion Suns: The Birth, Life, and Death of the Stars
Figure 9.2 (a) A detached binary. Both stars are clearly located within the
maximal permitted volume outlined by the broken curved line, (b) A
semidetached binary. The left star completely fills out its Roche volume. one just
about fills its volume ...
6
Relativistic Gravitation and Gravitational Radiation ...
Semidetached binary evolution We consider a compact (primary) star of mass MI
in an orbit of separation a with a non-compact secondary of mass MI- In all cases
of interest, tidal dissipation in the latter star keeps the binary orbit circular and ...
Jean-Alain Marck, Jean-Pierre Lasota,
1997
7
A Dictionary of Astronomy
The variable period and the emission lines that are sometimes detectable in its
spectrum are evidence for *mass transfer, indicating that the system is a *
semidetached binary. The eclipsing pair, which consists of a B8 dwarf and a K2
subgiant, ...
8
Evolutionary Processes in Interacting
Binary Stars
... it had become a semidetached binary, after RLOF. In a semi-detached binary
undergoing conservative case D mass transfer, after passing the critical mass
ratio (defined later), the loser would lose mass on its nuclear timescale. Since ...
Y. Kondo, R.F. Sisteró, R.S. Polidan,
1992
9
Binary and Multiple Stars as Tracers of Stellar Evolution: ...
... in fact observed. 289 Z. Kopal and J. Rahe (eds.), Binary and Multiple Stars as
Tracers of Stellar Evolution, 289-299. Copyright © 1982 by D. Reidel Publishing
Company. 2. Evolution from a detached or semidetached binary by angular XLIII.
International Astronomical Union. Colloquium, Z. KOPAL (Ed), Jürgen Rahe,
1982
10
Advances in Stellar Evolution
The model space densities of wide, close detached, and semidetached binary
degenerates are consistent with observations. Recent studies by Marsh and his
collaborators have significantly increased the number of known detached close ...
Robert T. Rood, Alvio Renzini,
1997